DOCSLIB.ORG

Download Preprint

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Figure 1 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 2 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 3 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 4 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 5 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 6 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 7 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 8 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 9 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 10 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 11 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 12 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 13 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 14 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS Figure 15 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS 1 Tectono-magmatic, sedimentary and hydrothermal history of Arsinoes and 2 Pyrrhae Chaos, Mars 3 Erica Luzzi1, Angelo Pio Rossi1, Cristian Carli2 and Francesca Altieri2 4 5 1Jacobs University, Bremen, Germany 6 2Inaf-IAPS Tor Vergata, Rome, Italy 7 Corresponding author: Erica Luzzi ([email protected]) 8 Key points 9 10 • We produced a morpho-stratigraphic map of Arsinoes and Pyrrhae Chaos, including the 11 volcanic grabens occurring throughout the study area; 12 • Spectral analyses of the light-toned deposits provide clues for sedimentary and 13 hydrothermal minerals; spectral analyses of the bedrock are indicative of basaltic 14 compositions; 15 • The observed volcano-tectonic surface features and the lack of evidences of any fluvial 16 activity suggest that magmatic processes might be primarily responsible for the collapse 17 of the chaotic terrain. 18 19 Abstract 20 Arsinoes and Pyrrhae Chaos are two adjacent chaotic terrains located east of Valles Marineris 21 and west of Arabia Terra, on Mars. In this work we produced a morpho-stratigraphic map of 22 the area, characterized by a volcanic bedrock disrupted into polygonal mesas and knobs 23 (Chaotic Terrain Unit) and two non-disrupted units. The latter present a spectral variation, 24 likely associated with hydrated minerals, and they are here interpreted as sedimentary units. 25 The reconstructed geological history of the area starts with the emplacement of the basaltic 1 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS 26 bedrock, followed by the collapse that caused the formation of the chaotic terrains. Since 27 evidences of volcano-tectonic activity are widespread across the area (e.g. fissure vents/graben, 28 radial and concentric systems of faults, y-shaped conjunctions, lava flows, pit chains), and an 29 intricate system of lava conduits is hypothesized for the occurrence of such features, we 30 propose the possibility that the whole collapse was caused primarily by volcano-tectonic 31 processes. In a late stage, after the end of the volcano-tectonic activity, a lacustrine/evaporitic 32 depositional environment could have set, with the deposition of the non-disrupted units. The 33 hydrated minerals found in the periphery of the Chaos could be the result of hydrothermal 34 alteration of the basaltic bedrock. 35 Keywords:Chaotic terrains; Mapping; Spectral analyses; Mars; Hydrothermal system. 36 Plain Language Summary 37 Chaotic terrains are peculiar features on Mars. They consist of broad regions characterized by a variable surface 38 disruption pattern of large polygonal blocks. Formation scenarios in the literature have always included a collapse, 39 possibly caused by a range of processes, all including water or hydrated compounds (magma-ice interactions, 40 melting of buried ice, groundwater pressure, etc.). In this work, we propose volcano-tectonic processes as 41 mechanism of formation for closed chaotic terrains. Additionally, our mineralogical analyses suggest that during 42 a late stage of the volcanic activity a hydrothermal system could have set. In such scenario hot water would have 43 risen from the subsurface through fractures created by the volcanic activity, evolving from eruptive to 44 hydrothermal. However, water would not have been directly involved in the initial collapse that formed the chaos. 45 1 Introduction 46 Arsinoes and Pyrrhae Chaos are two adjacent chaotic terrains, respectively centered at 7.8°S, 47 332°E and 10.3°S, 331.5°E (Fig. 1), a few tens of kilometres south of Aureum Chaos and a few 48 hundred kilometres SW of Aram Chaos, sharing with the latter many structural and 49 depositional characteristics. Several mechanisms of formation were proposed in literature to 2 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS 50 explain the nature of the putative collapse responsible for the disruption of the bedrock into 51 polygonal blocks that characterizes the chaotic terrains. The proposed scenarios include: i) a 52 major role played by groundwater and cryosphere, particularly linked to changes of pressure 53 within the aquifer that caused the disruption of the bedrock and subsequent water outflow 54 (Andrews-Hanna & Phillips, 2007; Carr, 1979; Harrison & Grimm, 2009; Rodriguez et al., 55 2005), ii) the occurrence of a buried ice lake that after melting would have caused fracturing 56 and catastrophic outflow (Manker & Johnson, 1982; Roda et al., 2014; Zegers et al., 2010), iii) 57 catastrophic destabilization of buried clathrates (Hoffman, 2000; Kargel et al., 2007), and iv) 58 magma-cryosphere/groundwater interactions (Chapman & Tanaka, 2002; Head & Wilson, 59 2007; Leask et al., 2006; Meresse et al., 2008; Wilson & Head III, 2002). Given the complexity 60 of the current geologic setting of Arsinoes and Pyrrhae Chaos, possibly augmented by an 61 extended time of erosion and mantling, a possible interaction between the proposed processes 62 (or singular contributions at different times) must also be considered. 63 In the present work we performed the morpho-stratigraphic mapping of Arsinoes and Pyrrhae 64 Chaos and a spectral analysis of the deposits. We propose a possible sequence of events to 65 explain the occurrence of the collapsed bedrock involving magmatic processes followed by an 66 aqueous depositional environment. 67 68 1.2 Regional setting 69 The first comprehensive description of chaotic terrains was made by Sharp et al. (1971) using 70 Mariner 6 imagery, followed by Sharp (1973) based on Mariner 9 data and Schultz et al. (1982) 71 based on Viking data. In this early stage of research, the main features of Martian chaotic 72 terrains were already clear and these areas were defined as deeply collapsed terrains disrupted 73 into an irregular pattern of tilted mesas and knobs, in some cases associated with outflow 3 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS 74 channels. The Chaotic Terrain Unit was first defined by Schultz and Rogers (1982) and then 75 with a refinement by Glotch & Christensen (2005) into three subunits: Fractured Plains, 76 Knobby Terrain and High Thermal Inertia Chaotic Terrain. The Chaotic Terrain Unit is 77 interpreted as the basaltic bedrock (Christensen et al., 2000; Glotch & Christensen, 2005) and 78 occurs over a large area including several other chaotic terrains such as Aureum, Aram, 79 Hydratoes, Aurorae, Chryse and Hydaspis Chaos. The age of the Chaotic Terrain Unit 80 according to Tanaka et al., (2014) is Middle Noachian, with younger Hesperian ages in the 81 internal portions of collapsed areas. With the collection of new compositional data from 82 THEMIS (Thermal Emission Imaging System), TES (Thermal Emission Spectrometer), 83 OMEGA (Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité) and CRISM 84 (Compact Reconnaissance Imaging Spectrometer for Mars), the investigations in literature 85 focused mainly on the sedimentary units lying on top of the basaltic bedrock. Several authors 86 analyzed the mineralogy of the layered sedimentary units occurring for example in Aram Chaos 87 (Catling & Moore, 2003; Christensen et al., 2001; Dobrea et al., 2008; Gendrin et al., 2005; 88 Glotch & Christensen, 2005; Lichtenberg et al., 2010; Liu et al., 2012; Massé et al., 2008; 89 Ormö et al., 2004), Aureum and Iani Chaos (Dobrea et al., 2008; Glotch & Rogers, 2007; 90 Sefton-Nash et al., 2012). Hematite deposits associated with monohydrated and polyhydrated 91 sulfates were spatially correlated with layered sedimentary units, separated by an unconformity 92 from the basaltic bedrock. The occurrence of hydrated sulfates and hematite allowed some 93 authors to assume that an aqueous and/or hydrothermal depositional environment must have 94 set after the collapse of the bedrock. The sedimentary layered deposits in Arsinoes Chaos were 95 not included in the previous studies, while in Pyrrhae Chaos the sedimentary deposits are not 96 observed at all. The lack of studies in this location emphasizes the need to expand our 97 knowledge of this area, providing a broader context on Martian chaotic terrains. 4 SUBMITTED TO JOURNAL OF GEOPHYSICAL RESEARCH: PLANETS 98 2 Data and methods 99 2.1 Data, processing and tools 100 The imagery used to perform the geological mapping is provided by the CTX (Context Camera) 101 (Malin et al., 2007) and HiRISE (High Resolution Imaging Science Experiment) (McEwen et 102 al., 2007) instruments onboard the MRO (Mars Reconnaissance Orbiter). One HRSC (High 103 Resolution Stereo Camera, on board Mars Express spacecraft) image was also used to observe
Recommended publications
  • Thermal Studies of Martian Channels and Valleys Using Termoskan Data

    Thermal Studies of Martian Channels and Valleys Using Termoskan Data

    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 99, NO. El, PAGES 1983-1996, JANUARY 25, 1994 Thermal studiesof Martian channelsand valleys using Termoskan data BruceH. Betts andBruce C. Murray Divisionof Geologicaland PlanetarySciences, California Institute of Technology,Pasadena The Tennoskaninstrument on boardthe Phobos '88 spacecraftacquired the highestspatial resolution thermal infraredemission data ever obtained for Mars. Included in thethermal images are 2 km/pixel,midday observations of severalmajor channel and valley systems including significant portions of Shalbatana,Ravi, A1-Qahira,and Ma'adimValles, the channelconnecting Vailes Marineris with HydraotesChaos, and channelmaterial in Eos Chasma.Tennoskan also observed small portions of thesouthern beginnings of Simud,Tiu, andAres Vailes and somechannel material in GangisChasma. Simultaneousbroadband visible reflectance data were obtainedfor all but Ma'adimVallis. We find thatmost of the channelsand valleys have higher thermal inertias than their surroundings,consistent with previousthermal studies. We show for the first time that the thermal inertia boundariesclosely match flat channelfloor boundaries.Also, butteswithin channelshave inertiassimilar to the plainssurrounding the channels,suggesting the buttesare remnants of a contiguousplains surface. Lower bounds ontypical channel thermal inertias range from 8.4 to 12.5(10 -3 cal cm-2 s-1/2 K-I) (352to 523 in SI unitsof J m-2 s-l/2K-l). Lowerbounds on inertia differences with the surrounding heavily cratered plains range from 1.1 to 3.5 (46 to 147 sr). Atmosphericand geometriceffects are not sufficientto causethe observedchannel inertia enhancements.We favornonaeolian explanations of the overall channel inertia enhancements based primarily upon the channelfloors' thermal homogeneity and the strongcorrelation of thermalboundaries with floor boundaries. However,localized, dark regions within some channels are likely aeolian in natureas reported previously.
  • Evidence for Volcanism in and Near the Chaotic Terrains East of Valles Marineris, Mars

    Evidence for Volcanism in and Near the Chaotic Terrains East of Valles Marineris, Mars

    43rd Lunar and Planetary Science Conference (2012) 1057.pdf EVIDENCE FOR VOLCANISM IN AND NEAR THE CHAOTIC TERRAINS EAST OF VALLES MARINERIS, MARS. Tanya N. Harrison, Malin Space Science Systems ([email protected]; P.O. Box 910148, San Diego, CA 92191). Introduction: Martian chaotic terrain was first de- ple chaotic regions are visible in CTX images (Figs. scribed by [1] from Mariner 6 and 7 data as a “rough, 1,2). These fractures have widened since the formation irregular complex of short ridges, knobs, and irregular- of the flows. The flows overtop and/or bank up upon ly shaped troughs and depressions,” attributing this pre-existing topography such as crater ejecta blankets morphology to subsidence and suggesting volcanism (Fig. 2c). Flows are also observed originating from as a possible cause. McCauley et al. [2], who were the fractures within some craters in the vicinity of the cha- first to note the presence of large outflow channels that os regions. Potential lava flows are observed on a por- appeared to originate from the chaotic terrains in Mar- tion of the floor as Hydaspis Chaos, possibly associat- iner 9 data, proposed localized geothermal melting ed with fissures on the chaos floor. As in Hydraotes, followed by catastrophic release as the formation these flows bank up against blocks on the chaos floor, mechanism of chaotic terrain. Variants of this model implying that if the flows are volcanic in origin, the have subsequently been detailed by a number of au- volcanism occurred after the formation of Hydaspis thors [e.g. 3,4,5]. Meresse et al.
  • Iani Chaos As a Landing Site for the Mars Science Laboratory. T. D. Glotch1, 1Jet Propulsion Laboratory, Cali- Fornia Institute of Technology

    Iani Chaos As a Landing Site for the Mars Science Laboratory. T. D. Glotch1, 1Jet Propulsion Laboratory, Cali- Fornia Institute of Technology

    Iani Chaos as a landing site for the Mars Science Laboratory. T. D. Glotch1, 1Jet Propulsion Laboratory, Cali- fornia Institute of Technology. [email protected] Iani Chaos, the source region of Ares Valles, is centered at ~342°E, 2°S. The chaotic terrain is widely- believed to have formed via the removal of subsurface water or ice, resulting in flooding at the surface, and the formation of Ares Vallis. Within Iani Chaos, de- posited stratigraphically above the chaotic terrain, are smooth, low-slope, intermediate-to-light-toned depos- its that are rich in a hydrated mineral that is most likely gypsum [1] as well as hematite[2-3] (Figure 1). Crystalline hematite and sulfates have been de- tected from orbit in numerous locations, including Me- ridiani Planum [4], Aram Chaos [1,5-6], Valles Marin- eris[5], and Aureum and Iani Chaos[2-3]. The MER Opportunity rover landed at Meridiani Planum and has shown that hematite is present as spherules that erode from a light-toned sulfate-rich outcrop. The MER team’s hypothesis of an ancient dune/interdune playa environment at Meridiani Planum[7] has been chal- lenged by both volcanic[8] and impact[9] models. A Figure 1. Map of hematite abundance in Iani Chaos. Hema- rover sent to one of the other locations rich in hematite tite abundance varies from ~5-20%. Based on OMEGA and sulfates will help to resolve the current debate and data[1], the presence of sulfate roughly correlates with that increase understanding of the role of ground and sur- of hematite.
  • Are We Martians? Looking for Indicators of Past Life on Mars with the Missions of the European Space Agency

    Are We Martians? Looking for Indicators of Past Life on Mars with the Missions of the European Space Agency

    CESAR Scientific Challenge Are we Martians? Looking for indicators of past life on Mars with the missions of the European Space Agency Teacher's Guide 1 Are we Martians? CESAR Scientific Challenge Table of contents: Didactics 5 Phase 0 18 Phase 1 20 Activity 1: Refresh concepts 21 Activity 2: Getting familiar with coordinates 21 Activity 2.1: Identify coordinates on an Earth map 21 Activity 2.2: The Martian zero meridian 24 Activity 2.3: Identify coordinates on a Martian map 25 Activity 2.4: A model of Mars 27 Activity 3: The origin of life 28 Activity 3.1: What is life? 28 Activity 3.2: Traces of extraterrestrial life 29 Activity 3.2.1: Read the following article 30 Activity 3.2.2: Read about Rosalind Franklin and ExoMars 2022 30 Activity 3.3: Experiment for DNA extraction 31 Activity 4: Habitable zones 31 Activity 4.1: Habitable zone of our star 31 Activity 4.2: Study the habitable zones of different stars 34 Activity 4.3: Past, present and future of water on Mars 37 Activity 4.4: Extremophiles 39 Activity 5: What do you know about Mars? 40 Activity 6: Scientific knowledge from Mars’ surface 41 Activity 6.1: Geology of Mars 41 Activity 6.2: Atmosphere of Mars 44 Activity 7: Mars exploration by European Space Agency 45 Activity 7.1: Major Milestones of the European Space Agency on Mars 50 Activity 8: Check what you have learnt so far 52 2 Are we Martians? CESAR Scientific Challenge Phase 2 53 Activity 9: Ask for a videocall with the CESAR Team if needed 54 Phase 3 56 Activity 10: Prepare the Mars landing 57 Activity 10.1: Get used to Google Mars.
  • Évolution De Molécules Organiques En Conditions Martiennes Simulées

    Évolution De Molécules Organiques En Conditions Martiennes Simulées

    Thèse de doctorat de l’Université Paris Est (UPE) Ecole doctorale Sciences, Ingénierie et Environnement (SIE) Évolution de molécules organiques en conditions martiennes simulées Expériences en laboratoire et en orbite basse terrestre sur la Station Spatiale Internationale Présentée par : Laura ROUQUETTE Sciences de l’Univers et Environnement Spécialité Astronomie, Astrophysique Sous la direction de : Pr. Hervé Cottin et Dr. Fabien Stalport Soutenue le 19 novembre 2018 Composition du jury : Sylvain BERNARD Chargé de Recherche Rapporteur Grégoire DANGER Maître de Conférences Rapporteur Antonella BARUCCI Astronome Examinatrice Frances WESTALL Directrice de Recherche Présidente Hervé COTTIN Professeur Directeur de thèse Fabien STALPORT Maître de Conférences Co-directeur de thèse 2 3 4 Remerciements En classe de 5ème, comme tous mes camarades, j’ai eu droit au classique rendez-vous d’orientation avec une conseillère. Elle m’a demandé ce que je voulais faire plus tard. Je lui ai répondu « astrophysicienne » et comme beaucoup d’adultes avant elle, et encore d’autres après elle, elle s’est un peu moquée de mon ambition. Elle m’a néanmoins expliqué que je devais passer mon brevet des collèges, faire un bac S, une licence, un master, puis un doctorat. La route a été longue depuis ce rendez-vous d’orientation de 5ème au collège Jolimont de Toulouse, et la liste des personnes à remercier pour ce grade de « docteur », obtenu quatorze ans plus tard, l’est également. Je vais donc essayer de n’oublier personne, mais probablement en vain. Tout d’abord, merci à mes parents d’avoir été là, du début à la fin. De m’avoir appris que beaucoup de choses étaient possibles avec du travail, de ne pas avoir fait taire mes ambitions, de m’avoir valorisée tout au long de ma vie.
  • Fluid-Deposited Fracture-Margin Ridges in Margaritifer Terra, Mars

    Fluid-Deposited Fracture-Margin Ridges in Margaritifer Terra, Mars

    Lunar and Planetary Science XLVIII (2017) 1185.pdf FLUID-DEPOSITED FRACTURE-MARGIN RIDGES IN MARGARITIFER TERRA, MARS. Rebecca. J. Thomas1, Sally Potter-McIntyre2 and Brian. M. Hynek1,3 1 LASP, University of Colorado, Boulder, CO 80309, USA, [email protected], 2 Southern Illinois University, Geology Department, Parkinson Lab Mailcode 4324, Carbondale, IL 62901, 3 Department of Geological Sciences, University of Colorado, 399 UCB, Boulder, CO 80309, USA. Introduction: Sites where mineral deposition oc- thermal inertia material are present superposing the curred in association with fluid flow emanating from light-toned unit, indicating its original presence over a the subsurface are excellent targets at which to seek larger proportion of the floor. The floor fill is cross-cut evidence for past life on Mars. This is because aqueous by multiple fractures up to 650 m wide. By analogy environments are favorable to life, and precipitated with other impact craters in the region, where exposure minerals have the potential to encase biosignatures, of light-toned brecciated material (LTBr) from beneath protecting them from degradation in the oxidizing envi- a dark capping unit is clearly associated with crater- ronment at the martian surface [1,2]. We report the floor fractures, we propose that erosion was accom- occurrence of ridges at the margins of broad fractures plished by fluid upwelling from these fractures. Chan- in Margaritifer Terra, and conduct morphological and nels carved into the crater rim are consistent with over- stratigraphic analysis of two key sites to determine spill of this fluid to the surrounding terrain. At the their probable mode of formation.
  • The Surface of Mars Michael H. Carr Index More Information

    The Surface of Mars Michael H. Carr Index More Information

    Cambridge University Press 978-0-521-87201-0 - The Surface of Mars Michael H. Carr Index More information Index Accretion 277 Areocentric longitude Sun 2, 3 Acheron Fossae 167 Ares Vallis 114, 116, 117, 231 Acid fogs 237 Argyre 5, 27, 159, 160, 181 Acidalia Planitia 116 floor elevation 158 part of low around Tharsis 85 floor Hesperian in age 158 Admittance 84 lake 156–8 African Rift Valleys 95 Arsia Mons 46–9, 188 Ages absolute 15, 23 summit caldera 46 Ages, relative, by remote sensing 14, 23 Dikes 47 Alases 176 magma supply rate 51 Alba Patera 2, 17, 48, 54–7, 92, 132, 136 Arsinoes Chaos 115, 117 low slopes 54 Ascreus Mons 46, 49, 51 flank fractures 54 summit caldera 49 fracture ring 54 flank vents 49 dikes 55 rounded terraces 50 pit craters 55, 56, 88 Asteroids 24 sheet flows 55, 56 Astronomical unit 1, 2 Tube-fed flows 55, 56 Athabasca Vallis 59, 65, 122, 125, 126 lava ridges 55 Atlantis Chaos 151 dilatational faults 55 Atmosphere collapse 262 channels 56, 57 Atmosphere, chemical composition 17 pyroclastic deposits 56 circulation 8 graben 56, 84, 86 convective boundary layer 9 profile 54 CO2 retention 260 Albedo 1, 9, 193 early Mars 263, 271 Albor Tholus 60 eddies 8 ALH84001 20, 21, 78, 267, 273–4, 277 isotopic composition 17 Alpha Particle X-ray Spectrometer 232 mass 16 Alpha Proton-ray Spectrometer 231 meridional flow 1 Alpheus Colles 160 pressure variations and range 5, 16 AlQahira 122 temperatures 6–8 Amazonian 277 scale height 5, 16 Amazonis Planitia 45, 64, 161, 195 water content 11 flows 66, 68 column water abundance 174 low
  • A Rare Premiere

    A Rare Premiere

    Press release date: 21 January 2008 Listings date: 15 March 2008 A RARE PREMIERE DOUBLE PIANO CONCERTO Glasgow 15 March 2008 Piano Duo, Philip Moore and Simon Crawford Philips will perform the world premiere of a new concerto for two pianos and orchestra on March 15th with the BBC Scottish Symphony Orchestra (BBCSSO) conducted by Martyn Brabbins at Glasgow City Halls. The new work, simply titled Double Concerto has been commissioned from German composer Detlev Glanert by the Borletti-Buitoni Trust (the Piano Duo was awarded a BBT fellowship in 2004) and the BBC SSO. Simon Crawford-Philips and Philip Moore formed the Piano Duo in 1995, as a result of meeting at the Royal Academy where they were both pupils of Hamish Milne and have won several awards and prizes as a duo as well as individually. Hamburg-born Detlev Glanert studied with Henze and has been composing since the age of 12. British audiences would best remember his highly acclaimed Proms debut in 2005 when the BBC Symphony Orchestra premiered his Theatrum Bestiarum. The Double Concerto’s inspiration was found on Mars: the composer was fascinated by the Pathfinder images of the planet and the physical features that had been given names from European mythology. Rather than the Martian landscape itself, it was the concept of man interpreting absolutely unknown landscapes with well known names that intrigued him. The concerto’s nine movements are therefore named after Martian landscape features, from Nirgal Vallis to Elysium Mons. Glanert explores the idea of double-play on a number of levels.
  • Preliminary Geologic Analysis of Sedimentary Deposits Exposed in Chaotic Terrains Within the Chryse Region on Mars

    Preliminary Geologic Analysis of Sedimentary Deposits Exposed in Chaotic Terrains Within the Chryse Region on Mars

    Preliminary geologic analysis of sedimentary deposits exposed in chaotic terrains within the Chryse region on Mars 1 1 1 2 German M. Sowe , E. Hauber , R. Jaumann , G. Neukum and the HRSC Co-Investigator Team 1 2 DLR Aerospace Center Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany ([email protected]), Remote Sensing of the Earth and Planets, Freie Universitaet Berlin, Germany Introduction Chaotic terrains on Mars are mainly located in the source regions of the outflow channels East of Valles Marineris. They are supposed to be formed by fluidisation of an incompetent layer underlying material that is more competent. Various states of disruption are observed especially in chasmata where some knobs are present. The High Resolution Stereo Camera (HRSC) on ESA`s Mars Express mission (MEX) provides 3D-images of the Martian surface in high resolution, while the spectrometer Observatoire pour la Minéralogie, l’Eau, les Glaces, et l’Activité (OMEGA/ MEX) produces data characterising the mineralogical composition of the surface. Very high-resolution Mars Orbiter Camera (MOC) images reveal the texture of the layers, whereas some physical properties of the surface layer can be derived from Thermal Infrared Imaging Spectrometer (THEMIS) night time-infrared data. We just started a project to use HRSC-, MOC, OMEGA-, THEMIS- and Mars Orbiter Laser Altimeter (MOLA)-data in order to analyse the stratigraphy of Interior Layered Deposits (ILDs) in the chaotic terrains, from Eos Chasma in the west to Aram Chaos in the east. The layers will be characterised by the following parameters: stratigraphic position and elevation, thickness, layer geometry, albedo, colour, physical properties, and chemical composition.
  • Water and Martian Habitability Results of an Integrative Study Of

    Water and Martian Habitability Results of an Integrative Study Of

    Planetary and Space Science 98 (2014) 128–145 Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Water and Martian habitability: Results of an integrative study of water related processes on Mars in context with an interdisciplinary Helmholtz research alliance “Planetary Evolution and Life” R. Jaumann a,b,n, D. Tirsch a, E. Hauber a, G. Erkeling c, H. Hiesinger c, L. Le Deit a,d, M. Sowe b, S. Adeli a, A. Petau a, D. Reiss c a DLR, Institute of Planetary Research, Berlin, Germany b Freie Universität Berlin, Institute of Geosciences, Berlin, Germany c Institut für Planetologie, Westfälische Wilhelms-Universität, Münster, Germany d Laboratoire de Planétologie et Géodynamique, UMR 6112, CNRS, Université de Nantes, Nantes, France article info abstract Article history: A study in context with the Helmholtz Alliance ‘Planetary Evolution and Life’ focused on the (temporary) Received 11 March 2013 existence of liquid water, and the likelihood that Mars has been or even is a habitable planet. Both Received in revised form geomorphological and mineralogical evidence point to the episodic availability of liquid water at the 10 February 2014 surface of Mars, and physical modeling and small-scale observations suggest that this is also true for Accepted 21 February 2014 more recent periods. Habitable conditions, however, were not uniform over space and time. Several key Available online 5 March 2014 properties, such as the availability of standing bodies of water, surface runoff and the transportation of Keywords: nutrients, were not constant, resulting in an inhomogeneous nature of the parameter space that needs to Mars be considered in any habitability assessment.
  • Modern Astronomy: Voyage to the Planets Lecture 4 the Red Planet

    Modern Astronomy: Voyage to the Planets Lecture 4 the Red Planet

    Modern Astronomy: Voyage to the Planets Lecture 4 Mars the Red Planet University of Sydney Centre for Continuing Education Autumn 2005 first spacecraft to reach Mariner 4 flyby 1965 Mars Mariner 6 flyby 1969 Mariner 7 flyby 1969 Mariner 9 orbiter There have been many Mars 5 USSR orbiter 1973 spacecraft sent to orbiter/lander Viking 1 Landed Chryse Planitia Mars over the past 1976-1982 orbiter/lander Viking 2 Landed Utopia Planitia few decades. Here are 1976-1980 the successful ones, Mars Global orbiter Laser altimeter with a description of Surveyor 1997-present the highlights of each Mars Pathfinder lander & rover 1997 Landed Ares Vallis mission. 2001 Mars orbiter Studying composition Odyssey 2001-present Mars Express/ ESA orbiter + lander Geology + atmosphere Beagle 2003–present Spirit & rovers Landed Gusev Crater & Opportunity 2003–present Meridiani The Face of Mars Basic facts Mars Mars/Earth Mass 0.64185 x 1024 kg 0.107 Radius 3397 km 0.532 Mean density 3.92 g/cm3 0.713 Gravity (equatorial) 3.71 m/s2 0.379 Semi-major axis 227.92 x 106 km 1.524 Period 686.98 d 1.881 Orbital inclination 1.85o - Orbital eccentricity 0.0935 5.59 Axial tilt 25.2o 1.074 Rotation period 24.6229 h 1.029 Length of day 24.6597 h 1.027 Mars is quite small relative to Earth, but in other ways is extremely similar. The radius is only half that of Earth, though the total surface area is comparable to the land area of Earth. It take nearly twice as long to orbit the Sun, but the length of its day and its axial tilt are very close to Earth’s.
  • Martian Geomorphology and Its Relation to Subsurface Volatiles

    Martian Geomorphology and Its Relation to Subsurface Volatiles

    MECA Special Session at LPSC XVII: MARTIAN GEOMORPHOLOGY AND ITS RELATION TO SUBSURFACE VOLATILES MECA MECA Special Session at LPSC XVII: MARTIAN GEOMORPHOLOGY AND ITS RELATION TO SUBSURFACE VOLATILES edited by Stephen M. Clifford, Lisa A. Rossbacher, and James R. Zimbelman Sponsored by The Lunar and Planetary Institute Hosted by The NASA/Johnson Space Center March 17, 1986 Lunar and Planetary Institute 3303 NASA Road 1 Houstot1, Texas 77058-4399 LPI Technical Report 87 -02 Compiled in 1987 by the LUNAR AND PLANETARY INSTITUTE The Institute is operated by Universities Space Research Association under Contract NASW-4066 with the National Aeronautics and Space Administration. Material in this document may be copied without restraint for library, abstract service, educational, or personal research purposes; however, republication of any portion requires the written permission of the authors as well as appropriate acknowledgment of this publication. This report may be cited as: Clifford S. M., Rossbacher L. A., and Zimbelman J. R., eds. (1987) MECA Special Session at LPSC XVII: Martian Geomorphology and its Relation to SubsurJace Volatiles. LPI Tech. Rpt. 87-{)2. Lunar and Planetary Institute, Houston. 51 pp. Papers in this report may be cited as: Author A. A. (1986) Title of paper. In MECA Special Session at LPSC XVI!: Martian Geomorphology and its Relation to SubsurJace Volatiles (S. M. Clifford et aI., eds.), pp. XX- YY. LPI Tech Rpt. 87-{)2. Lunar and Planetary Institute, Houston. This report is distributed by: LIBRARY/ INFORMATION CENTER Lunar and Planetary Institute 3303 NASA Road I Houston, TX 77058-4399 Mail order requestors will be invoicedJor the cost oJpostage and handling.